The Astrophysical Journal Letters最新文献_第6页

3D Radiation-hydrodynamical Simulations of Shadows on Transition Disks 过渡盘阴影的三维辐射流体力学模拟

The Astrophysical Journal Letters Pub Date : 2024-10-17 DOI: 10.3847/2041-8213/ad815f

Shangjia Zhang and Zhaohuan Zhu

{"title":"3D Radiation-hydrodynamical Simulations of Shadows on Transition Disks","authors":"Shangjia Zhang and Zhaohuan Zhu","doi":"10.3847/2041-8213/ad815f","DOIUrl":"https://doi.org/10.3847/2041-8213/ad815f","url":null,"abstract":"Shadows are often observed in transition disks, which can result from obscuring by materials closer to the star, such as a misaligned inner disk. While shadows leave apparent darkened emission as observational signatures, they have significant dynamical impact on the disk. We carry out 3D radiation-hydrodynamical simulations to study shadows in transition disks and find that the temperature drop due to the shadow acts as an asymmetric driving force, leading to spirals in the cavity. These spirals have zero pattern speed following the fixed shadow. The pitch angle is given by tan−1(cs/vϕ) (6° if h/r = 0.1). These spirals transport mass through the cavity efficiently, with α ∼ 10−2 in our simulation. Besides spirals, the cavity edge can also form vortices and flocculent streamers. When present, these features could disturb the shadow-induced spirals. By carrying out Monte Carlo radiative transfer simulations, we show that these features resemble those observed in near-infrared scattered light images. In the vertical direction, the vertical gravity is no longer balanced by the pressure gradient alone. Instead, an azimuthal convective acceleration term balances the gravity–pressure difference, leading to azimuthally periodic upward and downward gas motion reaching 10% of the sound speed, which can be probed by Atacama Large Millimeter/submillimeter Array line observations.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142486659","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Production Population of Impact Craters in the Chang’E-6 Landing Mare 嫦娥六号着陆区撞击坑的生成量

The Astrophysical Journal Letters Pub Date : 2024-10-17 DOI: 10.3847/2041-8213/ad821a

Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng and Pei Ma

{"title":"The Production Population of Impact Craters in the Chang’E-6 Landing Mare","authors":"Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng and Pei Ma","doi":"10.3847/2041-8213/ad821a","DOIUrl":"https://doi.org/10.3847/2041-8213/ad821a","url":null,"abstract":"The Chang’E-6 mission accomplished the first sample return from the lunar farside. Earlier crater population measurements estimated the model age of the landing mare to range from the Eratosthenian to Late Imbrian, both of which are underrepresented by earlier returned samples. Establishing a new calibration point for lunar impact flux based on isotopic ages of the samples is promising, but the representative crater density for the landing mare (i.e., spatial density of craters with D ≥ 1 km; N(1)) is equally important for this purpose, which lacks good constraints. After excluding the effects of background secondaries, crater equilibrium, and observational uncertainties on crater statistics, this work extracts production populations in different diameter ranges (∼200 m–2 km) from multiple subareas of the landing mare. Cross-validation of the production populations verifies that N(1) derived from direct measurements of craters with D ≥ 1 km in sketched areas are reliable, which is (2.01 ± 0.90) × 10−3 and (6.05 ± 2.71) × 10−3 km2 for the western and eastern mare, respectively.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142448869","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

On the 1/f Spectrum in Slow Solar Wind Turbulence: The Role of Alfvénicity 慢速太阳风湍流中的 1/f 谱：阿尔费尼科性的作用

The Astrophysical Journal Letters Pub Date : 2024-10-16 DOI: 10.3847/2041-8213/ad81f9

Mason Dorseth, Sofiane Bourouaine and Jean C. Perez

{"title":"On the 1/f Spectrum in Slow Solar Wind Turbulence: The Role of Alfvénicity","authors":"Mason Dorseth, Sofiane Bourouaine and Jean C. Perez","doi":"10.3847/2041-8213/ad81f9","DOIUrl":"https://doi.org/10.3847/2041-8213/ad81f9","url":null,"abstract":"The slow solar wind has been recently observed to have a number of intervals that are dominated by large-scale Alfvénic fluctuations, especially within 1 au, with similar turbulence characteristics to those found in fast wind streams, including a 1/f range. These results suggest that the slow solar wind exists in at least two flavors: the typical slow wind that generally does not exhibit a 1/f range and an Alfvénic wind that is more similar to fast wind streams. The Alfvénic slow wind is usually differentiated from the typical slow wind (not dominated by Alfvénic fluctuations) by the normalized cross helicity, σc. Values of ∣σc∣ near unity are associated with Alfvénic fluctuations, whereas values near zero are typically thought of as non-Alfvénic. This classification by cross helicity excludes the case of solar wind fluctuations dominated by balanced Alfvénic turbulence, i.e., the turbulence regime where there is equal energy flux of counterpropagating fluctuations propagating along the mean field. We use a large statistical analysis to isolate intervals of slow wind at 1 au in a 20 yr period of Wind data. These intervals are sorted into subsets corresponding to the type of slow wind via the mean values of their magnetic compressibility and cross helicity. Our analysis finds several intervals of low-cross-helicity slow wind dominated by balanced Alfvénic turbulence, which possess similar characteristics found in high-cross-helicity streams. Our results support the conclusion that a 1/f spectrum may be a property associated with streams dominated by Alfvénic turbulence, whether the turbulence is balanced or imbalanced.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142448452","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST? 连接高倍率和低倍率：我们用 JWST 观测到银河系的起源了吗？

The Astrophysical Journal Letters Pub Date : 2024-10-16 DOI: 10.3847/2041-8213/ad833d

Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou and Alessandro Marconi

{"title":"Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST?","authors":"Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou and Alessandro Marconi","doi":"10.3847/2041-8213/ad833d","DOIUrl":"https://doi.org/10.3847/2041-8213/ad833d","url":null,"abstract":"The recent JWST observation of the Firefly Sparkle at z = 8.3 offers a unique opportunity to link the high- and the low-z Universe. Indeed, the claim of it being a Milky Way (MW) type of assembly at the cosmic dawn opens the possibility of interpreting the observation with locally calibrated galaxy-formation models. Here, we use the a state-of-the-art MW-evolution model to perform forward modeling of our Galaxy's progenitors at high-z. We build a set of mock spectra for the MW building blocks to make predictions for JWST and to interpret the Firefly Sparkle observation. First, we find that the most massive MW progenitor becomes detectable in a deep survey like JADES from z ≈ 8.2, meaning that we could have already observed MW analogs that still need interpretation. Second, we provide predictions for the number of detectable MW progenitors in lensed surveys like the CAnadian NIRISS Unbiased Cluster Survey, and interpret the Firefly Sparkle as a group of MW building blocks. Both the number of detections and the observed NIRCam photometry are consistent with our predictions. By identifying the MW progenitors whose mock photometry best fits the data, we find bursty and extended star formation histories, lasting >150–300 Myr, and estimate their properties: Mh ≈ 108−9M⊙, M⋆ ≈ 106.2−7.5M⊙, SFR ≈ 0.04–0.20 M⊙ yr−1, and Zgas ≈ 0.04–0.24 Z⊙. Uncovering the properties of MW analogs at cosmic dawn by combining JWST observations and locally constrained models will allow us to understand our Galaxy's formation, linking the high- and low-z perspectives.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142448455","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star AT2023vto：来自一颗大质量恒星的异常发光氦潮汐破坏事件

The Astrophysical Journal Letters Pub Date : 2024-10-16 DOI: 10.3847/2041-8213/ad7eb8

Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome and Giacomo Terreran

{"title":"AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star","authors":"Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome and Giacomo Terreran","doi":"10.3847/2041-8213/ad7eb8","DOIUrl":"https://doi.org/10.3847/2041-8213/ad7eb8","url":null,"abstract":"We present optical/UV observations and the spectroscopic classification of the transient AT2023vto as a tidal disruption event (TDE) at z = 0.4846. The spectrum is dominated by a broad blueshifted He iiλ4686 emission line, classifying it as a member of the TDE-He class. The light curve exhibits a persistent blue color of g − r ≈ −0.4 mag, long rise, and decline timescale, with a large peak absolute magnitude of Mg ≈ −23.2, making it the most luminous of the classical optical TDEs (H, H+He, He) discovered to date by about 1.5 mag. We identify the host galaxy of AT2023vto in archival Pan-STARRS images and find that the transient is located at the galaxy center. Modeling the light curves of AT2023vto, we find that it resulted from the disruption of a ≈8 M⊙ star by a ≈107M⊙ supermassive black hole. The star mass is about 5 times larger than the highest star masses previously inferred in TDEs, and the black hole mass is at the high end of the distribution. AT2023vto is comparable in luminosity and timescale to some putative TDEs (blue featureless continuum), as well as to the mean of a recently identified population of ambiguous nuclear transients (ANTs). ANTs have been speculated to arise from tidal disruptions of massive stars, perhaps in active galactic nuclei, and AT2023vto may represent a similar case to ANTs but in a dormant black hole, thereby bridging the TDE and ANT populations. We anticipate that the Rubin Observatory/LSST will uncover similar luminous TDEs to z ∼ 3.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142448761","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b GJ 1214 b 厚气溶胶上可能存在的二氧化碳

The Astrophysical Journal Letters Pub Date : 2024-10-15 DOI: 10.3847/2041-8213/ad7fef

Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg and Marcia J. Rieke

{"title":"Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b","authors":"Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg and Marcia J. Rieke","doi":"10.3847/2041-8213/ad7fef","DOIUrl":"https://doi.org/10.3847/2041-8213/ad7fef","url":null,"abstract":"Sub-Neptune planets with radii smaller than Neptune (3.9 R⊕) are the most common type of planet known to exist in the Milky Way, even though they are absent in the solar system. These planets can potentially have a large diversity of compositions as a result of different mixtures of rocky material, icy material, and gas accreted from a protoplanetary disk. However, the bulk density of a sub-Neptune, informed by its mass and radius alone, cannot uniquely constrain its composition; atmospheric spectroscopy is necessary. GJ 1214 b, which hosts an atmosphere that is potentially the most favorable for spectroscopic detection of any sub-Neptune, is instead enshrouded in aerosols (thus showing no spectroscopic features), hiding its composition from view at previously observed wavelengths in its terminator. Here, we present a JWST NIRSpec transmission spectrum from 2.8 to 5.1 μm that shows signatures of CO2 and CH4, expected at high metallicity. A model containing both these molecules is preferred by 3.3σ and 3.6σ as compared to a featureless spectrum for two different data analysis pipelines, respectively. Given the low signal-to-noise of the features compared to the continuum, however, more observations are needed to confirm the CO2 and CH4 signatures and better constrain other diagnostic features in the near-infrared. Further modeling of the planet’s atmosphere, interior structure and origins will provide valuable insights about how sub-Neptunes like GJ 1214 b form and evolve.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142449734","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Discovery of the Binarity of Gliese 229B, and Constraints on the System's Properties 发现格利泽 229B 的二元性，以及对该系统特性的约束

The Astrophysical Journal Letters Pub Date : 2024-10-15 DOI: 10.3847/2041-8213/ad7714

Samuel Whitebook, Timothy D. Brandt, G. Mirek Brandt and Emily C. Martin

引用次数: 0

Very High-energy Gamma-Ray Episodic Activity of Radio Galaxy NGC 1275 in 2022–2023 Measured with MACE 用 MACE 测量射电星系 NGC 1275 在 2022-2023 年的超高能量伽马射线外显活动

The Astrophysical Journal Letters Pub Date : 2024-10-14 DOI: 10.3847/2041-8213/ad8083

S. Godambe, N. Mankuzhiyil, C. Borwankar, B. Ghosal, A. Tolamatti, M. Pal, P. Chandra, M. Khurana, P. Pandey, Z. A. Dar, S. Godiyal, J. Hariharan, Keshav Anand, S. Norlha, D. Sarkar, R. Thubstan, K. Venugopal, A. Pathania, S. Kotwal, Raj Kumar, N. Bhatt, K. Chanchalani, M. Das, K. K. Singh, K. K. Gour, M. Kothari, Nandan Kumar, Naveen Kumar, P. Marandi, C. P. Kushwaha, M. K. Koul, P. Dorjey, N. Dorji, V. R. Chitnis, R. C. Rannot, S. Bhattacharyya, N. Chouhan, V. K. Dhar, M. Sharma and K. K. Yadav

{"title":"Very High-energy Gamma-Ray Episodic Activity of Radio Galaxy NGC 1275 in 2022–2023 Measured with MACE","authors":"S. Godambe, N. Mankuzhiyil, C. Borwankar, B. Ghosal, A. Tolamatti, M. Pal, P. Chandra, M. Khurana, P. Pandey, Z. A. Dar, S. Godiyal, J. Hariharan, Keshav Anand, S. Norlha, D. Sarkar, R. Thubstan, K. Venugopal, A. Pathania, S. Kotwal, Raj Kumar, N. Bhatt, K. Chanchalani, M. Das, K. K. Singh, K. K. Gour, M. Kothari, Nandan Kumar, Naveen Kumar, P. Marandi, C. P. Kushwaha, M. K. Koul, P. Dorjey, N. Dorji, V. R. Chitnis, R. C. Rannot, S. Bhattacharyya, N. Chouhan, V. K. Dhar, M. Sharma and K. K. Yadav","doi":"10.3847/2041-8213/ad8083","DOIUrl":"https://doi.org/10.3847/2041-8213/ad8083","url":null,"abstract":"The radio galaxy NGC 1275, located at the central region of Perseus cluster, is a well-known very high-energy (VHE) gamma-ray emitter. The Major Atmospheric Cherenkov Experiment Telescope has detected two distinct episodes of VHE (E > 80 GeV) gamma-ray emission from NGC 1275 during 2022 December and 2023 January. The second outburst, observed on 2023 January 10, was the more intense of the two, with flux reaching 58% of the Crab Nebula flux above 80 GeV. The differential energy spectrum measured between 80 GeV and can be described by a power law with a spectral index of Γ = −2.90 ± 0.16stat for both flaring events. The broadband spectral energy distribution derived from these flares, along with quasisimultaneous low-energy counterparts, suggests that the observed gamma-ray emission can be explained using a homogeneous single-zone synchrotron self-Compton model. The physical parameters derived from this model for both flaring states are similar. The intermediate state observed between two flaring episodes is explained by a lower Doppler factor or magnetic field, which subsequently returned to its previous value during the high-activity state observed on 2023 January 10.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142440630","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Stacking X-Ray Observations of “Little Red Dots”: Implications for Their Active Galactic Nucleus Properties 对 "小红点 "的叠加 X 射线观测：活动星系核属性的含义

The Astrophysical Journal Letters Pub Date : 2024-10-13 DOI: 10.3847/2041-8213/ad7eba

Minghao Yue, Anna-Christina Eilers, Tonima Tasnim Ananna, Christos Panagiotou, Erin Kara and Takamitsu Miyaji

{"title":"Stacking X-Ray Observations of “Little Red Dots”: Implications for Their Active Galactic Nucleus Properties","authors":"Minghao Yue, Anna-Christina Eilers, Tonima Tasnim Ananna, Christos Panagiotou, Erin Kara and Takamitsu Miyaji","doi":"10.3847/2041-8213/ad7eba","DOIUrl":"https://doi.org/10.3847/2041-8213/ad7eba","url":null,"abstract":"Recent James Webb Space Telescope observations have revealed a population of compact extragalactic objects at z ≳ 4 with red near-infrared colors, which have been dubbed as “Little Red Dots” (LRDs). The spectroscopically selected LRDs exhibit broad Hα emission lines, which likely indicate that type I active galactic nuclei (AGNs) are harbored in the galaxies’ dust-reddened cores. However, other mechanisms, like strong outflowing winds, could also produce broad Hα emission lines, and thus, the nature of LRDs is still under debate. We test the AGN hypothesis for LRDs by stacking the archival Chandra observations of 34 spectroscopically selected LRDs. We obtain tentative detections in the soft (0.5–2 keV) and hard (2–8 keV) X-ray bands with 2.9σ and 3.2σ significance, and with 4.1σ significance when combining the two bands. Nevertheless, we find that the soft (hard) band 3σ upper limit is ∼1 dex (∼0.3 dex) lower than the expected level from the LX–LHα relation for typical type I AGNs. Our results indicate that AGN activity is indeed likely present in LRDs though these objects have significantly different properties compared to previously identified type I AGNs, i.e., LRDs may have intrinsically weak X-ray emissions. We find it difficult to explain the low LX/LHα ratios observed in LRDs solely by absorption. It is also unlikely that fast outflows have major contributions to the broad Hα lines. Our findings indicate that empirical relations (e.g., for black hole mass measurements) established for typical type I AGNs should be used with caution when analyzing the properties of LRDs.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142440175","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Clearing Timescale for Infrared-selected Star Clusters in M83 with HST 用 HST 测量 M83 中红外选择星团的清除时间尺度

The Astrophysical Journal Letters Pub Date : 2024-10-13 DOI: 10.3847/2041-8213/ad7ba9

Suyash Deshmukh, Sean T. Linden, Daniela Calzetti, Angela Adamo, Matteo Messa, Kathryn Grasha, Elena Sabbi, Linda Smith and Kelsey E. Johnson

{"title":"The Clearing Timescale for Infrared-selected Star Clusters in M83 with HST","authors":"Suyash Deshmukh, Sean T. Linden, Daniela Calzetti, Angela Adamo, Matteo Messa, Kathryn Grasha, Elena Sabbi, Linda Smith and Kelsey E. Johnson","doi":"10.3847/2041-8213/ad7ba9","DOIUrl":"https://doi.org/10.3847/2041-8213/ad7ba9","url":null,"abstract":"We present an analysis of Hubble Space Telescope data from Wide Field Camera 3 (WFC3)/Ultraviolet Imaging Spectrometer, WFC3/IR, and the Advanced Camera for Surveys, investigating the young stellar cluster (YSC) population in the face-on spiral galaxy M83. Within the field of view of the IR pointings, we identify 454 sources with compact F814W continuum and Paβ line emission with a S/N ≥ 3 as possible YSC candidates embedded in dust. We refine this selection to 97 candidates based on their spectral energy distributions, multiwavelength morphology, and photometric uncertainties. For sources that are detected in all bands and have mass >102.8M⊙ (53 sources), we find that by 2 Myr 75% of IR-selected star clusters have an AV ≤ 1 and that by 3 Myr the fraction rises to ∼82%. This evidence of early clearing implies that presupernova (pre-SN) feedback from massive stars is responsible for clearing the majority of the natal gas and dust that surround IR-selected star clusters in M83. Further, this result is consistent with previous estimates based on WFC3 observations and adds to the growing body of literature suggesting pre-SN feedback to be crucial for YSC emergence in normal star-forming galaxies. Finally, we find a weak correlation between the YSC concentration index and age over the first 10 Myr, which matches previous studies and indicates little or no change in the size of YSCs in M83 during their early evolution.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-10-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142431647","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0